1,071 research outputs found
Three-body treatment of the penetration through the Coulomb field of a two-fragment nucleus
On the basis of the Faddeev integral equations method and the Watson-
Feshbach concept of the effective (optical) interaction potential, the first
fully consistent three-body approach to the description of the penetration of a
charged particle through the Coulomb field of a two-particle bound complex
(composed of one charged and one neutral particles) has been developed. A
general formalism has been elaborated and on its basis, to a first
approximation in the Sommerfeld parameter, the influence of the nuclear
structure on the probability of the penetration of a charged particle (the
muon, the pion, the kaon and the proton) through the Gamow barrier of a
two-fragment nucleus (the deuteron and the two lightest lambda hypernuclei,
lambda hypertriton and lambda hyperhelium-5, has been calculated and studied.Comment: LaTeX, 30 pages, 4 eps figure
Shape parameters of Galactic open clusters
(abridged) In this paper we derive observed and modelled shape parameters
(apparent ellipticity and orientation of the ellipse) of 650 Galactic open
clusters identified in the ASCC-2.5 catalogue. We provide the observed shape
parameters of Galactic open clusters, computed with the help of a
multi-component analysis. For the vast majority of clusters these parameters
are determined for the first time. High resolution ("star by star") N-body
simulations are carried out with the specially developed GRAPE code
providing models of clusters of different initial masses, Galactocentric
distances and rotation velocities. The comparison of models and observations of
about 150 clusters reveals ellipticities of observed clusters which are too low
(0.2 vs. 0.3), and offers the basis to find the main reason for this
discrepancy. The models predict that after Myr clusters reach an
oblate shape with an axes ratio of , and with the major axis
tilted by an angle of with respect to the
Galactocentric radius due to differential rotation of the Galaxy. Unbiased
estimates of cluster shape parameters require reliable membership determination
in large cluster areas up to 2-3 tidal radii where the density of cluster stars
is considerably lower than the background. Although dynamically bound stars
outside the tidal radius contribute insignificantly to the cluster mass, their
distribution is essential for a correct determination of cluster shape
parameters. In contrast, a restricted mass range of cluster stars does not play
such a dramatic role, though deep surveys allow to identify more cluster
members and, therefore, to increase the accuracy of the observed shape
parameters.Comment: 13 pages, 12 figures, accepted for publication in Astronomy and
Astrophysic
THE INVARIANT PATTERNS OF THE INTERNAL PROTEINS OF PANDEMIC INFLUENZA VIRUSES
The purpose of the study was to find molecular recognition characteristics of pandemic strains of influenza A viruses and to find out whether avian strains are the probable cause of a new influenza pandemic. Computer analysis of the internal proteins (nucleoprotein, matrix protein M1 and M2 proteins polymerase complex PB1, PB2 and PA, non-structural protein NS2; because of the variability of the length the non-structural NS1 protein was excluded from the analysis) of influenza A virus pandemics in 1918 (H1N1), 1957 (H2N2), 1968 (H3N2), 1977 (H1N1) and 2009 (H1N1) strains was used for search of the invariant pattern primary structure. It was revealed that internal proteins of pandemic strains are characterized by the constancy of the number and positions of certain amino acids and the presence of extended invariant fragments. On the basis of these identified patterns of invariances in internal proteins it was possible to accurately identify pandemic strains in the control sample. Pandemic strains, divided by decades in their emergence and different composition of subtypes of hemagglutinin and neuraminidase (H1, H2, H3 and N1, N2), have strong relationship for their internal proteins, forming a special subset. This suggests that emergence of influenza A virus pandemic strains is related to convergence of their internal proteins to the detected pandemic invariants. To identify pandemic invariant patterns is enough to have the training set including strains of four pandemics (1918, 1957, 1968, 1977). Therefore the 2009–2010 pandemic influenza strain could be predicted at the earliest stage according to its genome and proteome sequencing. According to a comparative analysis, the internal proteins of avian strains H5N1 and H7N9, particularly their nucleoproteins, are not close to those of pandemic strains. This suggests that the threat of a new influenza pandemic, provoked by current circulating avian strains, is unlikely. Invariant patterns of pandemic strains can potentially be used to track pre-pandemic strains among circulating influenza A viruses and detect the formation of a possible trajectory of pandemic alert
Long-range behavior of the optical potential for the elastic scattering of charged composite particles
The asymptotic behavior of the optical potential, describing elastic
scattering of a charged particle off a bound state of two charged, or
one charged and one neutral, particles at small momentum transfer
or equivalently at large intercluster distance
, is investigated within the framework of the exact three-body
theory. For the three-charged-particle Green function that occurs in the exact
expression for the optical potential, a recently derived expression, which is
appropriate for the asymptotic region under consideration, is used. We find
that for arbitrary values of the energy parameter the non-static part of the
optical potential behaves for as
. From this we derive for the
Fourier transform of its on-shell restriction for the behavior , i.e.,
dipole or quadrupole terms do not occur in the coordinate-space asymptotics.
This result corroborates the standard one, which is obtained by perturbative
methods. The general, energy-dependent expression for the dynamic
polarisability is derived; on the energy shell it reduces to the
conventional polarisability which is independent of the energy. We
emphasize that the present derivation is {\em non-perturbative}, i.e., it does
not make use of adiabatic or similar approximations, and is valid for energies
{\em below as well as above the three-body dissociation threshold}.Comment: 35 pages, no figures, revte
Моделювання зіткнення літаків з використанням методики істотних вибірок
We introduce the model of movement of two conflicting aircrafts and state the problem, we apply the importance sampling technique and elaborate an algorithm of collision modeling based on normal distributions, a small simulation studyРассмотрена модель движения двух конфликтующих самолетов. Предложены методика важных выборок и алгоритм моделирования столкновения самолетов, основанный на нормальном распределенииРозглянуто модель руху двох конфліктуючих літаків. Запропоновано методику істотних вибірок і алгоритм моделювання зіткнення літаків, заснований на нормальному розподіл
XHIP-II: Clusters and associations
Context. In the absence of complete kinematic data it has not previously been
possible to furnish accurate lists of member stars for all moving groups. There
has been an unresolved dispute concerning the apparent inconsistency of the
Hipparcos parallax distance to the Pleiades.
Aims. To find improved candidate lists for clusters and associations
represented among Hipparcos stars, to establish distances, and to cast light on
the Pleiades distance anomaly.
Methods. We use a six dimensional fitting procedure to identify candidates,
and plot CMDs for 20 of the nearest groups. We calculate the mean parallax
distance for all groups.
Results. We identify lists of candidates and calculated parallax distances
for 42 clusters and 45 associations represented within the Hipparcos catalogue.
We find agreement between parallax distance and photometric distances for the
most important clusters. For single stars in the Pleiades we find mean parallax
distance 125.6 \pm 4.2 pc and photometric distance 132 \pm 3 pc calibrated to
nearby groups of similar in age and composition. This gives no reason to doubt
either the Hipparcos database or stellar evolutionary theory.Comment: Accepted for publication in Astronomy Letters, 10 pages, 2 fig
Mesoscopic molecular ions in Bose-Einstein condensates
We study the possible formation of large (mesoscopic) molecular ions in an
ultracold degenerate bosonic gas doped with charged particles (ions). We show
that the polarization potentials produced by the ionic impurities are capable
of capturing hundreds of atoms into loosely bound states. We describe the
spontaneous formation of these hollow molecular ions via phonon emission and
suggest an optical technique for coherent stimulated transitions of free atoms
into a specific bound state. These results open up new interesting
possibilities for manipulating tightly confined ensembles.Comment: 4 pages (two-columns), 2 figure
FlyBase 101 – the basics of navigating FlyBase
FlyBase (http://flybase.org) is the leading database and web portal for genetic and genomic information on the fruit fly Drosophila melanogaster and related fly species. Whether you use the fruit fly as an experimental system or want to apply Drosophila biological knowledge to another field of study, FlyBase can help you successfully navigate the wealth of available Drosophila data. Here, we review the FlyBase web site with novice and less-experienced users of FlyBase in mind and point out recent developments stemming from the availability of genome-wide data from the modENCODE project. The first section of this paper explains the organization of the web site and describes the report pages available on FlyBase, focusing on the most popular, the Gene Report. The next section introduces some of the search tools available on FlyBase, in particular, our heavily used and recently redesigned search tool QuickSearch, found on the FlyBase homepage. The final section concerns genomic data, including recent modENCODE (http://www.modencode.org) data, available through our Genome Browser, GBrowse
Renormalization of the Three-Body System with Short-Range Interactions
We discuss renormalization of the non-relativistic three-body problem with
short-range forces. The problem becomes non-perturbative at momenta of the
order of the inverse of the two-body scattering length, and an infinite number
of graphs must be summed. This summation leads to a cutoff dependence that does
not appear in any order in perturbation theory. We argue that this cutoff
dependence can be absorbed in a single three-body counterterm and compute the
running of the three-body force with the cutoff. We comment on relevance of
this result for the effective field theory program in nuclear and molecular
physics.Comment: 5 pages, RevTex, 4 PS figures included with epsf.sty, some clarifying
comments added, version to appear in Phys. Rev. Let
Global survey of star clusters in the Milky Way VI. Age distribution and cluster formation history
The all-sky Milky Way Star Clusters (MWSC) survey provides uniform and
precise ages and other parameters for a variety of clusters in the Solar
Neighbourhood. We construct the cluster age distribution, investigate its
spatial variations, and discuss constraints on cluster formation scenarios of
the Galactic disk during the last 5 Gyrs. Due to the spatial extent of the
MWSC, we consider spatial variations of the age distribution along
galactocentric radius , and along -axis. For the analysis of the age
distribution we use 2242 clusters, which all lie within roughly 2.5 kpc of the
Sun. To connect the observed age distribution to the cluster formation history
we build an analytical model based on simple assumptions on the cluster initial
mass function and on the cluster mass-lifetime relation, fit it to the
observations, and determine the parameters of the cluster formation law.
Comparison with the literature shows that earlier results strongly
underestimated the number of evolved clusters with ages Myr.
Recent studies based on all-sky catalogues agree better with our data, but
still lack the oldest clusters with ages Gyr. We do not observe a
strong variation in the age distribution along , though we find an
enhanced fraction of older clusters ( Gyr) in the inner disk. In contrast,
the distribution strongly varies along . The high altitude distribution
practically does not contain clusters with Gyr. With simple assumptions
on the cluster formation history, cluster initial mass function and cluster
lifetime we can reproduce the observations. Cluster formation rate and cluster
lifetime are strongly degenerate, which does not allow us to disentangle
different formation scenarios. In all cases the cluster formation rate is
strongly declining with time, and the cluster initial mass function is very
shallow at the high mass end. (abridged)Comment: 11 pages, 9 figures, accepted for publication in Astronomy and
Astrophysic
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